The condensational instability in the solar transition region and corona

Details The condensational instability in the solar transition region and corona The condensational instability in the solar transition region and corona

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...254..349o&link_type=abstract

Astrophysical Journal, Part 1, vol. 254, Mar. 1, 1982, p. 349-360. NASA-Navy-supported research.

Astronomy and Astrophysics

Astrophysics

52

Astronomical Models, Magnetohydrodynamic Stability, Plasma Dynamics, Solar Corona, Computerized Simulation, Linear Equations, Nonlinear Equations, Plasma Conductivity, Plasma Oscillations, Plasma Temperature

Scientific paper

The stability of plasmas at temperatures and densities typical of the solar transition region and corona is investigated using both a linear analysis and nonlinear time-dependent numerical simulations. Growth rates, decay rates, and oscillation frequencies of the perturbations determined from the linear analysis are in excellent agreement with the simulations. The nonlinear regime is characterized by a bifurcation of the plasma into a cool dense condensation surrounded by a hot tenuous corona. The condensation may then be accelerated by forces in the plasma such as those arising from gravity or differential heating. Finally, the results of the detailed simulation show that the transition region is a dynamically stable structure which is the result of the nonlinear evolution of the condensational instability.

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